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J/ApJ/630/381       Mid-IR imaging in ρ Oph                 (Barsony+, 2005)

A mid-infrared imaging survey of embedded young stellar objects in the ρ Ophiuchi cloud core. Barsony M., Ressler M.E., Marsh K.A. <Astrophys. J., 630, 381-399 (2005)> =2005ApJ...630..381B
ADC_Keywords: Infrared sources ; Interstellar medium ; Stars, pre-main sequence Keywords: infrared: stars - ISM: individual (ρ Ophiuchi Cloud) - planetary systems: protoplanetary disks - stars: formation - stars: pre-main-sequence - surveys Abstract: Results of a comprehensive, new, ground-based mid-infrared imaging survey of the young stellar population of the ρ Ophiuchi cloud are presented. Data were acquired at the Palomar 5m and at the Keck 10m telescopes with the MIRLIN (Mid-InfraRed Large-well Imager) and LWS (Long Wavelength Spectrometer centered at 12.5µm) instruments, at 0.5" and 0.25" resolutions, respectively. Of 172 survey objects, 85 were detected. Among the 22 multiple systems observed, 15 were resolved and their individual component fluxes determined. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table2.dat 111 231 Mid-infrared fluxes for ρ Oph sources table3.dat 129 37 Mid-infrared variables in Ophiuchus table4.dat 132 176 ρ Oph source properties table5.dat 71 39 Mid-infrared observations of known binary/multiple systems in Ophiuchus
See also: J/ApJS/112/109 : Rho Oph Near-IR Positions and Photometry (Barsony+, 1997) J/ApJ/438/813 : Stellar population in ρ Oph cloud core (Strom+, 1995) J/AJ/130/1733 : Optical spectroscopy of ρ Oph stars (Wilking+, 2005) Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 13 A13 --- BKLT Source designations (G1) 15 A1 --- n_BKLT Note on BKLT (1) 17- 34 A18 --- OName Alias or other name 36 A1 --- n_OName Note on OName (1) 38- 39 I2 h RAh ? Hour of Right Ascension (J2000) 41- 42 I2 min RAm ? Minute of Right Ascension (J2000) 44- 48 F5.2 s RAs ? Second of Right Ascension (J2000) 50 A1 --- DE- Sign of the Declination (J2000) 51- 52 I2 deg DEd ? Degree of Declination (J2000) 54- 55 I2 arcmin DEm ? Arcminute of Declination (J2000) 57- 60 F4.1 arcsec DEs ? Arcsecond of Declination (J2000) 62- 63 A2 --- l_F10.8um [≤] Upper limit flag on F10.8um (3σ) 65- 71 F7.4 Jy F10.8um ? The 10.8µm flux 73- 74 A2 --- l_F12.5um [≤] Upper limit flag on F12.5um (3σ) 76- 80 F5.3 Jy F12.5um ? The 12.5mum flux (2) 82- 86 F5.3 Jy F12.5um2 ? Second 12.5mum flux (2) 88- 97 A10 "DD/MM/YYYY" ObsDate Observation date 99-111 A13 --- Tel The Telescope/Instrument used
Note (1): Flag on BKLT, defined as follows: 4 = Spectroscopically determined background giant (Luhman & Rieke 1999ApJ...525..440L); 5 = The secondary in the DoAr24E system is an Infrared Companion discovered by Chelli et al. (1988A&A...207...46C). 6 = WL16 and its extended PAH & VSG disk are thoroughly discussed in Ressler & Barsony (2003ApJ...584..832R); the aperture photometry presented here was measured in r=4" and r=3.75" circular apertures, for the data of 24 April 1996 and 30 June 1998, respectively. 7 = The combined flux of the WL20 triple system is listed here. See Ressler & Barsony (2001AJ....121.1098R) for a thorough discussion of this system. Individual source positions for each component are from Barsony, Greene, & Blake (2002ApJ...572L..75B). 8 = Our chop/nod directions and separations were poorly placed with respect to the WL3, WL4, WL5, & GY244 asterism. Hence, we quote an upper limit for WL5 derived from the average values for undetected sources for 24 April 1996, instead of measuring an upper limit directly from the co-added data for this source. Note (2): In general, the 12.5um fluxes were measured in a 0.72" aperture (as per Table 1). The 12.5um flux was measured with a 0.7" and a 2" aperture for 5 objects, WL12, WL22, GY292, IRS48, and GY352, in columns F12.5um and F12.5-2, respectively. These observations were obtained with LWS on Keck I on 29 June 1999.
Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
1- 13 A13 --- BKLT Source designations (G1) 14 A1 --- n_BKLT [p] primary 16 A1 --- f_BKLT Flag on BKLT (1) 18- 33 A16 --- OName Alias or other name 35- 36 A2 --- l_MIR [≤] Upper limit flag on MIR 37- 41 F5.3 Jy MIR ? The MIRLIN flux (2) 43- 48 F6.4 Jy e_MIR ? Uncertainty in MIR 50 A1 --- l_F10.8um Upper limit flag on F10.8um 51- 56 F6.3 Jy F10.8um ? ISOCAM 10.8µm flux 58- 62 F5.3 Jy e_F10.8um ? Uncertainty in F10.8um 64 A1 --- f_F10.8um Flag on F10.8um (1) 66- 70 F5.3 Jy LWS ? The LWS flux (12.5um) 72- 76 F5.3 Jy e_LWS ? Uncertainty in LWS 78- 82 F5.3 Jy F12.5um ? ISOCAM 12.5µm flux 84- 88 F5.3 Jy e_F12.5um ? Uncertainty in F12.5um 90 A1 --- f_F12.5um Flag on F12.5um (1) 92- 97 F6.3 Jy PGB1 ? Previous Ground-Based flux in MIR (N-band) 99-103 F5.3 Jy e_PGB1 ? Uncertainty in PGB1 105 A1 --- f_PGB1 Flag on PGB1 (1) 107-110 F4.2 Jy PGB2 ? Previous Ground-Based flux in MIR (N-band) 112-115 F4.2 Jy e_PGB2 ? Uncertainty in PGB2 117 A1 --- f_PGB2 Flag on PGB2 (1) 119-122 F4.2 Jy PGB3 ? Previous Ground-Based flux in MIR (N-band) 124-127 F4.2 Jy e_PGB3 ? Uncertainty in PGB3 129 A1 --- f_PGB3 Flag on PGB3 (1)
Note (1): Flag, defined as follows: 1 = Flux from Table 2 of Wilking, Lada, & Young (1989ApJ...340..823W) 2 = Flux from Table 4 of Rydgren, Strom, & Strom (1976ApJS...30..307R) 3 = Flux from Table 1 of Lada & Wilking (1984ApJ...287..610L) 4 = Flux from Table 2 of Elias (1978ApJ...224..453E) 5 = Flux from Table 1 of Greene et al. (1994ApJ...434..614G) 6 = The SR24 system is a hierarchical triple, with a 6.0" separation between the primary, SR24S (=BKLT J162658-244534), and the secondary, SR24N (= BKLT J162658-244529), which itself consists of a 0.20" separation binary. Although SR24S and SR24N were unresolved by ISOCAM, previous ground-based observations did resolve these components. N-band fluxes for SR24S are 0.78±0.029Jy (Wilking, Lada, & Young, 1989ApJ...340..823W) and 2.28±0.21Jy (Greene et al., 1994ApJ...434..614G), to be compared with MIRLIN fluxes of 2.01Jy and 1.66Jy for SR24S on 26 June 1997 and 7 June 1998, respectively. N-band fluxes for SR24N are 1.17±0.029 Jy (Wilking, Lada, & Young, 1989ApJ...340..823W) and 1.67±0.16Jy (Greene et al., 1994ApJ...434..614G), to be compared with the MIRLIN flux of 1.40Jy for both dates of observation. Therefore, we can conclude that it is the single, primary star in this system, SR24S, which is the mid-infrared variable. 7 = WL20 (= BKLT J162715-243843) is a triple system, which was noted as highly variable in unresolved ISOCAM 6.7µm measurements. The previously published N-band flux for the WL20 system from ground-based measurements was 0.180±0.03Jy (Lada & Wilking, 1984ApJ...287..610L). Our observations resolve the triple system in the mid-infrared, and show that it is the "infrared companion", WL20S, which is the mid-infrared variable (see Table 2). 8 = ISOCAM data from Wilking et al. (2001ApJ...551..357W). Note (2): There is a second observation of WLY64 of 0.48±0.005.
Byte-by-byte Description of file: table4.dat
Bytes Format Units Label Explanations
1- 13 A13 --- BKLT Source designations (G1) 15- 40 A26 --- OName Alias or other name 42 A1 --- f_OName Flag on OName (1) 44- 48 F5.2 mag Kmag ? The K band magnitude 50- 51 A2 --- l_H-K [≥ ] Lower limit flag on H-K 52- 55 F4.2 mag H-K ? The (H-K) color index 57- 58 A2 --- l_Sp+Index [≤] Upper limit flag on Sp+Index 59- 63 F5.2 --- Sp+Index ? The IR spectral index (2) 65- 70 A6 --- SED Spectral energy distribution class (4) 72-102 A31 --- rK Spectroscopically determined K-band veiling and source (3) 104-132 A29 mag AV The V band extinction and source (3)
Note (1): Flag on OName, defined as follows: 3 = The nature of WLY64 remains to be clarified, although it is listed as an FU Ori candidate source by Luhman & Rieke, 1999ApJ...525..440L. 4 = Spectroscopically determined background giant (Luhman & Rieke, 1999ApJ...525..440L); Note (2): Calculated between 2.2µm and either 10.8µm or 12.5µm, as available from Table 2. Note (3): From Luhman & Rieke (1999ApJ...525..440), unless otherwise indicated. B02 = Boogert et al. (2002ApJ...570..708B); BA92 = Bouvier & Appenzeller (1992A&AS...92..481B); BGB02 = Barsony, Greene, & Blake (2002ApJ...572L..75B); DJW03 = Doppmann, Jaffe, & White (2003AJ....126.3043D); D04 = Doppmann (2004, private communication); GL97 = Greene & Lada (1997AJ....114.2157G); GL02 = Greene & Lada (2002AJ....124.2185G); GM95 = Greene & Meyer (1995ApJ...450..233G); PGS03 = Prato, Greene, & Simon (2003ApJ...584..853P); W94 = Walter et al. (1994AJ....107..692W); W01 = Wilking et al. (2001ApJ...551..357W); WGM99 = Wilking, Greene, & Meyer (1999AJ....117..469W) Note (4): F.S. = flat spectrum. The SED class indicates an importance of circumstellar matter, interpreted as an evolutionary sequence: -- Class I object is one in which the central YSO has attained its initial main-sequence mass but is still surrounded by a remnant infall envelope and accretion disk; -- Class II object is surrounded by an accretion disk; -- Class III object has only a remnant, or absent, accretion disk.
Byte-by-byte Description of file: table5.dat
Bytes Format Units Label Explanations
1- 13 A13 --- BKLT Source designations (G1) 15- 26 A12 --- OName Alias or other name 28- 29 I2 h RAh ? Hour of Right Ascension (J2000) 31- 32 I2 min RAm ? Minute of Right Ascension (J2000) 34- 38 F5.2 s RAs ? Second of Right Ascension (J2000) 40 A1 --- DE- Sign of the Declination (J2000) 41- 42 I2 deg DEd ? Degree of Declination (J2000) 44- 45 I2 arcmin DEm ? Arcminute of Declination (J2000) 47- 50 F4.1 arcsec DEs ? Arcsecond of Declination (J2000) 52- 56 A5 --- Type Multiplicity type (1) 58- 63 F6.3 arcsec Sep ? Separation (2) 65- 69 F5.1 deg PA ? Position angle (3) 71 A1 --- Res? Resolved in Mid-IR?
Note (1): System type, defined as follows: B = Binary; SpB = Spectroscopic Binary; T = Triple; Q = Quadruple. Note (2): The WL20W, WL20S, and WL20E separations are measured E-W, S-W, and S-E. The uncertainties in IRS 2 and VSSG 27 are both ±0.03. Note (3): PAs are E of N, measured from the primary at K, except for IRS34, where the primary is at N, since no resolved K band data exist. The uncertainty in the IRS 2 and VSSG 27 PA's are ±4 and ±1, respectively.
Global notes: Note (G1): From Barsony et al. (1997, Cat. J/ApJS/112/109). BKLT JHHMMSS+DDMMSS in Simbad.
History: * 04-Jan-2006: From electronic version of the journal * 07-Aug-2007: BKLT 162623-242603 transformed into BKLT 162623-244311 (tables 2 and ) BKLT 162730-242755 transformed into BKLT 162730-242744 (table4)
(End) Greg Schwarz [AAS], Marianne Brouty [CDS] 04-Jan-2006
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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